Bolometric correction

Mathematically, such a calculation can be expressed: BC = M_\text{bol} - M_v The bolometric correction for a range of stars with different spectral types and groups is shown in the following table: The bolometric correction is large and negative both for early type (hot) stars and for late type (cool) stars. The former because a substantial part of the produced radiation is in the ultraviolet, the latter because a large part is in the infrared. For a star like the Sun, the correction is only marginal because the Sun radiates most of its energy in the visual wavelength range. Bolometric correction is the correction made to the absolute magnitude of an object in order to convert an object's visible magnitude to its bolometric magnitude. Alternatively, the bolometric correction can be made to absolute magnitudes based on other wavelength bands beyond the visible electromagnetic spectrum. For example, and somewhat more commonly for those cooler stars where most of the energy is emitted in the infrared wavelength range, sometimes a different value set of bolometric corrections is applied to the absolute infrared magnitude, instead of the absolute visual magnitude. Mathematically, such a calculation could be expressed: BC_K = M_\text{bol} - M_k Where MK is the absolute magnitude value and BCK is the bolometric correction value in the K-band. ==Setting the correction scale==

The bolometric correction scale is set by the absolute magnitude of the Sun and an adopted (arbitrary) absolute bolometric magnitude for the Sun. Hence, while the absolute magnitude of the Sun in different filters is a physical and not arbitrary quantity, the absolute bolometric magnitude of the Sun is arbitrary, and so the zero-point of the bolometric correction scale that follows from it. This explains why classic references have tabulated apparently mutually incompatible values for these quantities. Although bolometric magnitudes have been in use for over eight decades, there have been systematic differences in the absolute magnitude-luminosity scales presented in various astronomical references with no international standardization. This has led to systematic differences in bolometric correction scales. When combined with incorrect assumed absolute bolometric magnitudes for the Sun this can lead to systematic errors in estimated stellar luminosities. Many stellar properties are calculated based on stellar luminosity, such as radii, ages, etc. IAU 2015 Resolution B2 proposed an absolute bolometric magnitude scale where M_\text{bol} = 0 corresponds to luminosity , with the zero point luminosity chosen such that the Sun (with nominal luminosity ) corresponds to absolute bolometric magnitude M_{\text{bol}_{\rm Sun}} = 4.74. Placing a radiation source (e.g. star) at the standard distance of 10 parsecs, it follows that the zero point of the apparent bolometric magnitude scale m_\text{bol} = 0 corresponds to irradiance f_{o} = 2.518 021 002... \times 10^{-8} \mathrm{ W/m^2}, where the nominal total solar irradiance measured at 1 astronomical unit (1361 W/m2) corresponds to an apparent bolometric magnitude of the Sun of m_{\text{bol}_{\rm Sun}} = -26.832. A similar IAU proposal in 1999 (with a slightly different zero point, tied to an obsolete solar luminosity estimate) was adopted by IAU Commissions 25 and 36. However it never reached a General Assembly vote, and subsequently was only adopted sporadically by astronomers in the literature. ==See also==